The High Energy cosmic Radiation Detection (HERD) facilityDetection (HERD) facility

onboard China’s Space Stationp

Shuang-Nan Zhang ( )zhangsn@ihep.ac.cn

Center for Particle Astrophysics

Institute of High Energy PhysicsChinese Academy of Sciences

1/45

Beijing

2/45

3/45

IHEP Campus Map

Electron-Positron ColliderElectron Positron Collider

4/45

Research in IHEP: >1300 fulltime staff

S iScience goals Fundamental structure of matter and evolution of the

universe

Total funding in

Collider, Synchrotron,

g2012: ~140 Meu

Multi-discipline

Underground lab, high-altitude cosmic ray observatory, space iPlatform instruments

5/45

Tibet High Altitude Cosmic ray Observatory

Sea Level and Underground Exp.CMS Daya Bay

Space ProjectsAMS, CE, HXMT

POLAR DAMPE SVOM

Cosmic-ray ObservatoryYBJ AS , ARGO

LHAASOCMS, Daya-Bay

Dark Matter SearchPOLAR, DAMPE, SVOM

SEMS, XTP, HERD

IHEP Center for Particle

160 fulltime staff scientists andTotal funding in for Particle

Astrophysicsscientists and engineers

g2012: ~14 Meu

High Energy Cosmic-rayCharged Particles

Gravity & CosmologyCompact ObjectsCharged Particles,

Neutrinos, Gamma-raysExplosive Phenomena

GRB,SN&SNR

Compact ObjectsGalaxy, Cluster

CMB,

BH&NS accretion6/45

China’s Space Station Program• Three phases

– 1st phase: so far 7 Chinese astronauts have been1 phase: so far 7 Chinese astronauts have been sent out and returned back successfully; many space science research has been done. C l t d f llCompleted successfully.

– 2nd phase: spacelab: docking of 3 spaceships with astronauts delivering and installing scientificwith astronauts delivering and installing scientific instruments. 1st launch on Sept. 29, 2011.

– 3rd phase: spacestation: several large– 3 phase: spacestation: several large experimental cabins with astronauts working onboard constantly. 1st launch ~2018.y

International collaborations on space science research have been and will continue to be an important part.p p

7/45

Cosmic Lighthouse Program: China’s Space Station

Candidate Projects Main Science Topics

Large scale imaging and Dark energy dark matter distribution large scalespectroscopic survey facility (approved)

Dark energy, dark matter distribution, large scale structure of the universe

Dark matter properties cosmic ray compositionHERD (concept) Dark matter properties, cosmic ray composition, high energy electron and gamma-raysSoft X-ray-UV all sky monitor X-ray binaries, supernovae, gamma-ray bursts, active galactic (?) nuclei, tidal disruption of stars by supermassive black holes

X-ray polarimeter (?) Black holes, neutron stars, accretion disks, supernova remnants

Galactic warm-hot gas spectroscopic mapper (?)

The Milky Way, interstellar medium, missing baryons in the Universe

High sensitivity solar high Solar flares, high energy particle acceleration mechanism, space g y genergy detector (?)

, g gy p , pweather

Infrared spectroscopic survey telescope (?) Stars, galaxies, active galactic nucleitelescope (?)

8/45

Gamma-raybackground

HERD l tHERD electron

protonHe

Dark matter particle

9/359/45

AMS02

Weight 8,500 kgVolume 64 m3Cost $1.5 billion ( i d)(estimated)

10/45

Recent AMS02 Results: electrons

11/45

Recent AMS02 Results: protons

12/45

Recent AMS02 Results: Heliums

13/45

Beyond AMS: DAMPE

The detector is consisted of 4 parts:Top scintillatorsTop scintillatorsSi tracker (5 layers)BGO calorimeterBGO calorimeterNeutron detector

e: 0.3m2sr@200GeV@

p: 0.12 m2sr@100TeV

14/45

Beyond AMS: CALET

Ch

0.12 m2sr@100TeV

I i

Charge Detector

Imaging Calorimeter

Total Absorption Calorimeter

32 cm

15/45

Expected CALET proton and He spectra after 5 years of observation

Maestro, ICRC 2013

16/45

Expected CALET measurement of more abundant heavy nuclei

Maestro, ICRC2013

17/45

Beyond AMS: CREAM

0.2 m2Sr@100 TeV for protonfor protonOn ISS

18/45

Science goals and requirements for HERD

Science goals Mission requirementsDark matter search

R1: Better statistical measurements of e/ between 100 GeV to 10 TeV

Origin of Galactic

R2: Better spectral and composition measurements of CRs betweenGalactic

Cosmic raysmeasurements of CRs between 300 GeV to PeV* with a large geometrical factorgeometrical factor

Secondary science: monitoring of GRBs, microquasars, Blazars andother transientsother transients.*Complimentary to key LHAASO science

19/45

HERD Cosmic Ray Capability Requirement

P ( ~ 1)He ( ~ 4)( )L ( ~ 8)M ( ~ 14)H ( ~ 25)Model 1 Model 2 ( )VH ( ~ 35) Fe ( ~ 56)

Model 2

PeV PeV

Except for L, up to PeV spectra feasible with

PeV PeVCREAM CREAM feasible with

GF~2-3 in ~years: 0;

2 yr

)

CREAM CREAM

discriminate between models

N(E

>E0

HERD HERD

models.TeV TeV

20/45

Old Baseline design of HERDThe detector is consisted of 4 parts:

Micro silicon striptracker

PWO or BGO

ECAL: Electromagneticcalorimeter

PWO or BGO

HCAL: Hadronic

Graphite target

HCAL: Hadroniccalorimeter: 3D CsI stackwith ICCD readout

Only 1.2m2sr for cosmic rayscosmic rays

21/45

New Baseline design of HERD

22/45

Characteristics of all components

type size X0, unit main functionst k Si 70 2 X0 7 Chtracker(top)

Si strips

70 cm 70 cm

2 X0 7 x-y(W foils)

ChargeEarly showerTracksTracks

tracker4 sides

Si strips

65 cm 50 cm

-- 3 x-y Nucleon TrackCharge4 sides strips 50 cm Charge

CALO LYSO b

63 cm 63

55 X0

3 cm 3

e/ energylcubes 63 cm

63 cmX03

3 cm 3 cm

nucleon energye/p separation

23/45

Why LYSO detectors?

Crystal CsI(Na) BGO PWO LYSODensity (g/cm3) 4.51 7.13 8.3 7.41 X0 (cm) 1.86 1.12 0.89 1.14Rm (cm) 3.57 2.23 2.00 2.071 (cm) 39.3 22.8 20.7 20.9Decay time (ns) 690 300 30 40Light yield (%) 88 21 0.3 85Light yield (%) 88 21 0.3 85

crystal + wls fiber

24/45

Proton energy resol. vs. detector thicknessGF@

100 TeV GF 3.0GF 2.0

100 TeV2.6

63*63*63cm 77*77*42cm 90*90*31cm63 63 63cm3 nucl.inter.length,20% resolution

77 77 42cm2 nucl.inter.length,30% resolution

90 90 31cm1.5 nucl.inter.length,50% resolution

Total detector weight: 2000 kg25/45

HERD reconstruction vs. energy resol.

Under the weight limitation of 2 tons, resolution is more important for spectralresolution is more important for spectral

reconstruction, based on the current design.26/45

Simulation results: energy resolutions

27/45

e/p separation (TMVA)

8 parameters8 parameters

28/45

e/p separation (TMVA)

6.0 10-6

29/45

HERD Geometrical Factor

~10XDAMPE ~20XDAMPE

30/45

Expected performance of HERD(electron) energy range tens of GeV-10TeV

nucleon energy range up to PeVnucleon energy range up to PeV

angular resol. (silicon) 0.1o

nucleon charge resol. (silicon) 0.1-0.15 c.u

(electron) energy resolution 1%@200GeVproton energy resolution 20%

e/p separation power 10-6

electron geometrical factor 3.1 m2sr@200 GeV

proton geometrical factor 2 3 m2sr@100 TeVproton geometrical factor 2.3 m sr@100 TeV

31/45

performance comparisonX0( ) E/E

for ee/psep.

e GFm2sr@

p GFm2sr@@

200GeV@

100TeVHERD (2020) 55(3) 1% 10-6 3.1 2.3Fermi (2008) 10 12% 10-3 0.9 --AMS02 (2011) 17 2% 10-6 0.12 --DAMPE (2015) 31 1% 10-4 0.3 --ISS-CREAM (2015) 20(1.5) -- -- -- 0.2( ) ( )

HERD can improve by at least 10X for electrons and 20X for cosmic rays over previous missions: this is necessary since it will operate much later.

32/45

HERD sensitivity to gamma-ray line

HERD 1 yr

PAMELA: 2006-2016 CALET: 2015-2020; AMS: 2011-2021;PAMELA: 2006 2016 CALET: 2015 2020; AMS: 2011 2021; DAMPE: 2015-2020; Fermi: 2008-2018; HERD: 2020-2021

33/45

HERD electron detection capability: 2021

HERD 1 yr

HERD 1 yry

Predicted spectrum Signal to Noise RatioPredicted spectrum Signal to Noise Ratio

34/45

HERD proton (nucleon) detection capability

HERD2020 20222020-2022CREAM2015 20202015-2020DAMPE2015 2020

HERD 2 yr

2015-2020CREAM 5 yr

But CREAM is planned to operate only for several

DAMPE 5 yronly for several months on ISS.

35/45

New calorimeter readout technique

Direct Coupling

PD, APD, SiPM:Complicated system, high power consumption

MAPMT SiPM: highMAPMT, SiPM: high power consumptionCCD: No single photon detectionEMCCD, EBCCD: no ns gate controlgate controlICCD: no above problems, but premature

Wavelength shifterfiber readout problems, but premature

36/45

An example

2.5 cm CsI(Na): ~ 188 p.e. for a passing muon

Sun, X. L. and et al. (2011). "A Digital Calorimeter for Dark Matter Search in Space." Journal of Physics: Conference Series 293(1): 012038.

37/45

Test set-up and results

2 2 6 granular CsI with fibers Taper +Imaging2 2 6 granular CsI with fibers sandwiched between two detectors

Taper +Imaging Intensifier + ICCD

ICCD image of typical muon events

38/45

Concept of ICCD readout system

Cathode Triggered I t ifi

Optical Coupler High frame rate and large format CCD

Intensifier

39/45

Two types of couplingRelay mirrors Taper

Single unit: weight of 18.393 kg, size size of 176 670(mm)size size of 176 670(mm)

Technology development funded by XIOPM, CAS and NSFC.ec o ogy de e op e t u ded by O , C S a d S CLooking for collaborators in Italy.

40/45

ICCD readout R&D

41/45

Current status of HERD• The mission concept (science goals with

requirements) has been selected, not in competition q ) pwith other missions.

• The design concept has been reviewed on Feb. 29,The design concept has been reviewed on Feb. 29, 2012, together with all other proposals in all fields.

• Technical review for mission selection may happen• Technical review for mission selection may happen anytime.La nch in 2018 2020• Launch in 2018-2020.

42/45

1st HERD workshop, Oct.17-18, 2012, IHEP, Beijing

Roberto Battiston et al. participated via video-con.43/45

The HERD Team• Current Chinese member institutions

– Institute of High Energy Physics, Chinag gy y ,– Purple Mountain Observatory, China– Xi’an Institute of Optical and Precision Mechanics, China– University of Science and Technology of China

• Current international member institutions (tentative)– University of Geneva, Switzerland– Università di Pisa and INFN, Italy– IAPS/INAF, Italy– University of Florence and INFN Firenze, Italy

f /– University of Perugia/Trento and INFN, Italy– University of Bari and INFN, Italy

KTH S d– KTH, Sweden

44/45

Possible contributions from INFN?• Mission concept and design of HERD

detectorsdetectors• Silicon trackers: similar to Italian contribution

to DAMPE• CALO: joint development• CALO: joint development• Additional detectors for

complementarities/redundancies• Anything else is also welcome!Anything else is also welcome!

45/45